The interaction of the stellar wind of massive stars with the ISM
produces gas nebulae witnessing the release of energy, momentum and
heavy chemical elements which enriched their local ambient
medium [1]}.
The classical picture for stellar wind-ISM interaction is that
of [2]} and it consists of a several parsec-scale
structured circumstellar bubbles surrounding massive stars.
The circumstellar medium of Wolf-Rayet stars is different, as many of
them display unusual smaller-scale ring-like gas nebulae detected in
H\(\alpha \)  and infrared, both in the Milky Way, see [3]}
and [4]}, and in the Magellanic
Clouds [5]}, [6]}, [7]}, [8]}, [9]}, respectively. A classification
of circumstellar structures around Wolf-Rayet stars arose from that
studies [10]}, [5]}, [12]}, [4]}, [14]}, [15]}.
Several follow-up surveys deepened and completed these observations in the
southern hemisphere, see [16]} and [17]}.
Wolf-Rayet nebulae entered the X-rays domain with
Asca [18]}
Rosat and
Chandra [19]},
XMM-Newton [20]}
observations from their (shocked) stellar winds witnessing
emission of optically-thin high temperature plasma.
More recently, a radio non-thermal synchrotron counterpart of the stellar
wind bubble of a Wolf-Rayet ring nebula indicated that these circumstellar
nebulae are the site of particles accelelration [21]}.
This accumulation of observations motivates the present numerical efforts
aiming at understanding the peculiar vicinity of young Wolf-Rayet stars.
